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Revisiting Disc-Jet Coupling in Black Hole X-ray Binaries: On the Nature of Disc Dynamics and Jet Velocity

T0 review · 4 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read Surveying 16 outbursts of 13 black hole X-ray binaries, the paper reports that type-A QPOs consistently show negative time lags regardless of source inclination, precede radio flares, and signal jet ejection, while type-B QPOs coincide…

desk verdict The QPO lag–flare census is worth a careful look, but the jet velocities are vitiated by an algebra error in Eq. (10). read the letter →

arxiv 2507.03644 v1 pith:G6HU6IQF submitted 2025-07-04 astro-ph.HE

Sreetama Das Choudhury (IITG) , Bhuvana G. R. (IAS) , Santabrata Das (IITG) , Anuj Nandi (URSC) This is my paper
classification astro-ph.HE
keywords blackholeX-raybinariesquasi-periodicoscillationstimelagscoronageometryjetejectionrelativisticjetsradio-X-raycorrelationaccretionstates
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper surveys sixteen outbursts of thirteen black hole X-ray binaries, combining X-ray timing and spectra with quasi-simultaneous radio data, to test how the corona changes as jets are launched. It reports a systematic pattern: type-C QPOs have inclination-dependent time lags, type-A QPOs always show negative lags and tend to precede radio flares, and type-B QPOs coincide with the flares. The authors interpret this as the corona shrinking radially and then elongating vertically during the transition from the hard intermediate state to the soft intermediate state, with type-B QPOs tracing a compact or vertically extended corona that resembles a jet base. They further estimate that jets in the soft intermediate state are moderately relativistic, at velocities >0.3–0.8c.

What carries the argument

The argument is carried by the time lag of each QPO type—the Fourier phase difference between the 2–6 keV and 6–15 keV lightcurves at the QPO frequency—used as a geometric probe of the corona. A positive lag is read as soft photons being Compton up-scattered in an extended corona before reaching the observer, while a negative lag is read as hard photons being reprocessed back into the disc, an effect that grows when the corona is small or the viewing angle is high. On the jet side, the machinery is the minimum-energy synchrotron formula for a radio-emitting blob, Doppler-corrected and equated through Equation (9) to a fraction of the accretion power, with that fraction set by the change in normalized Comptonized flux between successive X-ray observations around a flare.

What would settle it

Measure the proper motion of the radio ejecta during the soft intermediate state in a source whose velocity is predicted here (for example 4U 1543-47 or XTE J1752-223) and compare it with the paper's Table 3; a resolved speed clearly outside the predicted range would rule out the flux-change identification, while a single outburst with type-A QPOs appearing only after the radio flare peak would undercut the precursor claim.

Watch

Extended reading notes

Core claim

The central claim is that the sequence of QPO types encodes the geometry of the corona leading up to jet ejection. For thirteen sources the authors find that type-C QPOs, seen in harder states, show positive lags for low-inclination systems and negative lags for high-inclination systems, consistent with a large radially extended corona. Type-A QPOs appear near the state transition with negative lags of about 1–10 ms in every source regardless of inclination, and in several outbursts they show up before the radio flare, identifying them as precursors of jet ejection. Type-B QPOs, observed in the soft intermediate state with lower Comptonized flux, coincide with the radio flares and show positive lags in low-inclination sources and mixed lags in high-inclination sources, which the authors read as evidence for a radially compact or vertically elongated corona. Finally, using a minimum-energy jet model normalized to measured proper-motion speeds, the paper estimates jet velocities above 0.3–0.8c during the soft intermediate state, and concludes that the strong radio–X-ray correlation indicates accretion-powered jets.

Load-bearing premise

The jet velocities rest on the assumption that the decrease in normalized Comptonized flux between two X-ray observations around a radio flare measures the fraction of accretion power carried into the jet; if that flux change instead reflects a change in the accretion rate, the reported speeds do not follow.

Editorial extensions

If this is right

  • Type-A QPOs can serve as a practical early warning that a transient jet is about to be launched, enabling coordinated multi-wavelength follow-up.
  • The sign of the type-C QPO lag can be used to infer the inclination of a binary, or the radial extent of its corona, in sources without dynamical inclination measurements.
  • Type-B QPOs with positive lags identify a vertically elongated corona at the jet base, linking a timing signature directly to jet geometry.
  • Moderate SIMS jet velocities imply only modest Doppler boosting, changing how intrinsic radio luminosities should be estimated for intermediate-state jets.
  • The correlation between jet velocity and X-ray luminosity found in this sample suggests that accretion rate, rather than spin, is the main driver of jet speed.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The identification of the Comptonized flux change with the fraction of accretion power carried into the jet could be tested directly in a source with simultaneous X-ray and radio monitoring by separating thermal and Comptonized spectral components at high cadence; if the Comptonized flux drop tracks the radio lightcurve on timescales shorter than the accretion timescale, the outflow interpretation
  • If the precursor role of type-A QPOs holds up in future outbursts, it suggests that the jet launch itself modifies the corona, and that the delay between type-A and type-B QPOs may measure the vertical growth time of the jet base.
  • The log–log slope of about 0.33 between jet velocity and X-ray luminosity found here is a candidate scaling for jet-launching models and could be tested against theoretical predictions for radiatively inefficient accretion flows.
  • An analogous lag-sign ordering might be searched for in X-ray data of active galactic nuclei, where type-C-like low-frequency QPOs are observed, to see whether the geometry sequence is universal.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

4 major / 5 minor

Summary. The paper presents a spectro-temporal study of 16 outbursts from 13 black hole X-ray binaries, combining RXTE, HXMT, and AstroSat X-ray data with radio observations from the literature. The authors classify type-A, type-B, type-C, and type-C* QPOs, measure their time lags as a function of source inclination, and associate type-A QPOs with pre-radio-flare epochs and type-B QPOs with the flaring epochs. They argue that the corona evolves from a radially extended to a vertically elongated structure across the type-C-to-type-B transition. In the second half of the paper, they estimate black hole spins by continuum fitting and derive jet velocities by equating a minimum-energy radio-blob power with an assumed fraction of the accretion power, obtaining velocities in the range 0.3-0.8 c during the soft intermediate state.

Significance. If the empirical QPO-lag-inclination pattern holds, the paper would provide a useful phenomenological map connecting QPO subtypes, coronal geometry, and jet ejection, and the assembled lag measurements across many sources would be a valuable reference. The paper is also honest in stating some limitations, particularly in Section 6.3. However, the quantitative jet-velocity claim is not robust: the accretion-rate formula in Equation (10) has a self-contradictory dependence on radiative efficiency, and the epsilon values in Table 3 are either calibrated to the very velocities being predicted or identified with flux changes in a way the authors themselves call 'overly simplistic.' Since the headline '0.3-0.8 c' result depends on this chain, the central quantitative claim is currently not established.

major comments (4)
  1. [Section 5.2, Eq. (10)] Equation (10) places eta_acc in the numerator of the accretion-rate formula, but the stated relation L_x = eta_acc * Mdot * c^2 requires Mdot to be proportional to F_x D^2 / (eta_acc * c^2). With eta_acc ~ 0.1, the formula underestimates Mdot by roughly an order of magnitude (in addition to a missing 4 pi factor in the flux-to-luminosity conversion). Because Equation (9) gives beta proportional to (epsilon * Mdot)^(7/9), this error changes every beta in Table 3 by a factor of several and can push entries such as the 0.96-0.98 value for XTE J1752-223 above unity. The authors must correct Equation (10) and recompute the table before the velocity claims can be assessed.
  2. [Section 5.2 and Table 3] The epsilon values used to predict beta are not determined independently. For H1743-322 (2003 and 2009), XTE J1550-564, MAXI J1535-571, and XTE J1752-223 (F4), epsilon is chosen so that Equation (9) reproduces previously measured proper-motion velocities; the same epsilon convention is then applied to all other sources. Since beta is a monotone function of epsilon in Equation (9), agreement with the known velocities is partially by construction. The additional identification of epsilon with Delta F_nth is acknowledged in Section 6.3 to be 'overly simplistic,' but that caveat applies directly to the entries in Table 3, so the stated velocity range of 0.3-0.8 c is not independently established.
  3. [Section 5.2, Eqs. (6)-(9)] Equating the minimum-energy synchrotron power of a radio blob, W_min/t, with the kinetic jet power (1/2) eta_jet epsilon Mdot c^2 is a strong model assumption. W_min is a minimum total energy content of synchrotron-emitting plasma, not necessarily the jet kinetic power, and the adopted values eta_jet = 0.1 and k = 2 or 3 are fixed without a sensitivity analysis. Because beta depends on the 7/9 power of the resulting power ratio, plausible variations in these parameters could shift the headline velocities by tens of percent, and the paper should quantify this uncertainty before presenting 0.3-0.8 c as a precise result.
  4. [Section 4.3 and Figs. 6-7] The central empirical claim that type-A QPOs show negative lags independent of inclination and that type-B QPOs coincide with radio flares rests on manual QPO classification and on a small number of sources, with four high-inclination systems (XTE J1550-564, Swift J1727.8-1613, H1743-322 2003, and GRO J1655-40) explicitly listed as exceptions to the type-C lag-inclination trend. The paper should provide a per-source table of lag signs with uncertainties and a systematic treatment of the exceptions rather than setting them aside, especially because the claimed 'regardless of inclination' property of type-A QPOs is based on only 26 detections across the sample.
minor comments (5)
  1. [Section 3.1, Eq. (5)] The time-lag formula should read delta_t(j) = arg[C(j)] / (2 pi nu_j); as written, delta_t(j) = C(j) / (2 pi nu_j) is a complex quantity, not a real time delay.
  2. [Abstract and Section 2.1] The abstract lists the GX 339-4 outbursts as 2002, 2006, and 2010, while Section 2.1 and Table 1 refer to 2002, 2007, and 2010; the year 2006 appears to be a typo and should be corrected consistently.
  3. [Table 1] The 4U 1543-47 row lists the outburst year as 2004, but the text and Section 4.2 consistently describe the 2002 outburst; this should be made consistent.
  4. [Figure 10 caption] The caption refers to 'Swift J1727.8-0127,' whereas all other parts of the paper use Swift J1727.8-1613; the figure caption should be corrected.
  5. [Figure 9] The high-inclination correlation coefficients are quoted after excluding GRO J1655-40, but the figure does not state why this source is excluded; a brief justification should be given in the text or caption.

Circularity Check

2 steps flagged · score 6.0 of 10

Type-A/type-B QPO lag phenomenology is independent, but the quantitative jet velocities (Table 3) and the LX–β correlation reduce by construction: ε is calibrated to proper-motion β or set equal to ΔFnth, and Eq. (9) then maps that assumed ε back into β.

  1. fitted input called prediction [Section 5.2, Eqs. (7)–(10), Table 3 and Fig. 10]
    "Using these, we estimate ε ∼ 0.10 for 2003 outburst and 0.01 for 2009 outburst. For the 1998 outburst of XTE J1550−564, Hannikainen et al. (2009) reported the jet velocity β ≥ 0.8 that holds for ε ≥ 0.06. For MAXI J1535−571, β is reported as ∼ 0.69 (Russell et al. 2019), that corresponds to ε ≥ 0.12. ... For these sources, the predicted values of ε are in good agreement with the difference between the normalized Comptonized fluxes (Fnth) of successive observations during radio flares."

    Equation (9) forces β to be a function of ε once Mdot, η_jet, and the radio power are fixed. The paper first inverts proper-motion β measurements for H1743−322, XTE J1550−564, MAXI J1535−571, and XTE J1752−223 to obtain ε ≈ 0.01–0.12, then adopts ε = ΔFnth for other sources and solves Eq. (9) again for β. The Table 3 β values are therefore not independent measurements or first-principles predictions; they are the algebraic image of the adopted ε and the assumed η_jet ≈ 0.1. For the calibration sources, agreement with observed β is tautological; for the remaining sources, the reported β ≳ 0.3–0.8c range is contingent on the unverified identification ε = ΔFnth rather than on an independent constraint on jet speed.

  2. self definitional [Section 6.3, Fig. 13, with Eqs. (7), (9), and (10)]
    "Furthermore, we investigate the relationship between jet velocity (β) and bolometric X-ray luminosity (LX) during SIMS, where LX is generally higher than in HIMS. ... The Pearson correlation coefficient∼ 0.52 indicates a moderate positive correlation, suggesting that higher X-ray luminosity (equivalently mass accretion rate) is associated with faster jet velocities (β) during SIMS."

    β is not measured in Fig. 13; it is solved by equating Eq. (7) (L_jet ∝ β^(9/7) times radio observables) with Eq. (9) (L_jet = (1/2)η_jet ε Mdot c^2), where Eq. (10) gives Mdot ∝ L_X. Thus β^(9/7) is proportional to ε Mdot by construction, so a positive LX–β regression is largely baked into the model through the assumed accretion-to-jet power transfer. Presenting this regression as evidence that 'higher X-ray luminosity ... is associated with faster jet velocities' therefore partially rediscovers the ansatz of Eq. (9) rather than testing it independently. The independent empirical content in this section is the observed radio–X-ray luminosity correlation, not the model-generated β–LX correlation.

full rationale

The spectro-temporal analysis of QPO types, time lags, and their relation to source inclination is data-driven and self-contained: the type-A negative-lag pattern, the type-B/flare association, and the four coronal-geometry configurations are interpretations of directly measured lags and fluxes, not outputs of a fitted jet model. The circularity is confined to the quantitative jet-velocity chain. First, ε is either calibrated to known proper-motion β values or identified with ΔFnth, and Eq. (9) then returns β from that assumed ε; Table 3's 'predicted' velocities are therefore model outputs, not independent predictions, and the 0.3–0.8c claim inherits the ε = ΔFnth assumption. Second, the LX–β correlation in Fig. 13 largely follows from the assumed L_jet ∝ ε Mdot scaling in Eq. (9), so it is partially self-confirming. The paper itself concedes in Section 6.3 that 'the assumption that the changes in normalized Comptonized flux during radio flaring events directly correspond to ε may be overly simplistic, as these flux variations could also reflect intrinsic changes in the accretion rate, rather than solely the outflow.' Separately, Eq. (10) appears to place η_acc in the numerator, whereas L_x = η_acc Mdot c^2 would place it in the denominator; this is a serious correctness risk that would shift all Table 3 β values, but it is not itself a circularity. Overall, the central QPO-lag findings remain independent, but the paper's quantitative jet-velocity result and the β–LX correlation reduce substantially by construction, giving a partial-circularity score of 6.

Assumptions & free parameters 7 free parameters · 8 assumptions · 0 invented entities

The empirical lag pattern depends on the reliability of QPO typing and on the standard physical interpretation of lag sign. The jet velocities add a heavier load: epsilon, eta_jet, k, spectral index, rise time, spin, distance and mass all enter. Epsilon is the most fragile because it is estimated from flux changes that could be caused by accretion rate variations, as the authors themselves note.

free parameters (7)
  • epsilon (jet energy fraction) = 0.002 to 0.122 per flare (Table 3)
    Estimated from the change in normalized Comptonized flux across radio flares, or calibrated to proper-motion jet velocities for H1743-322, XTE J1550-564, MAXI J1535-571 and XTE J1752-223 F4. It directly controls the predicted jet velocity in Equation (9).
  • eta_jet (jet radiative efficiency) = 0.1 (assumed)
    Assumed constant in Equation (9) following Fender (2001a); chosen by hand and not measured; scales the inferred jet kinetic power and hence beta.
  • ejecta index k = 2 in HIMS, 3 in SIMS
    Chosen by hand from Fender et al. (2004, 2009); changes the Doppler correction in Equation (8) and therefore the inferred beta.
  • radio spectral index alpha = varies by source, not fully tabulated
    Used to normalize radio fluxes to 5 GHz in Equation (1); taken from the compiled radio literature for each source.
  • continuum-fit black hole spin a_k = 0.32 to 0.83 for nine sources (Table 2)
    Fitted with kerrbb2 for nine sources; spins for the other four are adopted from reflection-modeling literature. Spin sets the radiative efficiency eta_acc that enters Equation (10) and hence beta.
  • rise time t = interval between selected X-ray and radio observations
    Chosen as the gap between the X-ray observation used for Mdot and the radio flare; enters Equation (7) and affects the minimum-energy jet luminosity.
  • hardening factor f_col = 1.4 to 2.0
    Assumed range in continuum fitting; contributes systematic uncertainty in spin and eta_acc.
assumptions (8)
  • standard math Kerr ISCO radius and specific energy formulas used for eta_acc are correct.
    Invoked in Section 5.2 via Bardeen et al. (1972) and Thorne (1974); standard general relativity, not tested in this paper.
  • domain assumption QPO types A, B, C and C* as classified by the authors correspond to the standard definitions in the literature.
    Classifications are made by inspection of PDS shapes and parameters; see Section 3.1 and Figures 2 to 6.
  • domain assumption Positive lag indicates inverse Comptonization and negative lag indicates reprocessing or down-scattering.
    Used throughout Section 6.1 to interpret time lags as coronal geometry; cites Reig et al. (2000), Uttley et al. (2014) and others.
  • domain assumption Radio flare times mark the moment of jet ejection.
    Used to associate type-A and type-B QPOs with jet onset; based on previous literature such as Fender et al. (2004), but not directly confirmed for every source.
  • domain assumption The minimum-energy synchrotron estimate in Equation (6) captures the true energy of the ejected plasma blob.
    Required for Equation (7); assumes equipartition and spherical geometry, standard but unverified for these sources.
  • ad hoc to paper epsilon equals the change in normalized Comptonized flux between successive observations.
    Introduced in Section 5.2 and acknowledged as possibly overly simplistic in Section 6.3; no independent derivation is provided.
  • ad hoc to paper eta_jet = 0.1 and k = 2 or 3 depending on state.
    Assumed constants in Equations (8) and (9); not measured in this paper.
  • domain assumption Distances, masses, inclinations and literature spins used in Tables 1 and 2 are correct.
    Taken from cited references; systematic errors in these values would propagate directly into the accretion rate and beta estimates.

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Pith. "Pith review of Revisiting Disc-Jet Coupling in Black Hole X-ray Binaries: On the Nature of Disc Dynamics and Jet Velocity." pith.science (2026). https://pith.science/paper/G6HU6IQF

@misc{pith2026250703644,
  author       = {Pith},
  title        = {Pith review of: Revisiting Disc-Jet Coupling in Black Hole X-ray Binaries: On the Nature of Disc Dynamics and Jet Velocity},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/G6HU6IQF}},
  note         = {Machine review of arXiv:2507.03644}
}
abstract

We perform a comprehensive wide-band ($3-100$keV) spectro-temporal analysis of 13 outbursting BH-XRBs, using data (quasi)simultaneous with radio observations to unravel the complex disc-jet connection. RXTE observations are analyzed for XTEJ1859+226, GX339-4 (2002, 2006, and 2010 outbursts), 4U1543-47, H1743-322 (2003 and 2009 outbursts), XTEJ1550-564, XTEJ1752-223, XTEJ1650-500, SwiftJ1753.5-0127, XTEJ1748-288, and GROJ1655-40. For SwiftJ1727.8-1613 and MAXIJ1535-571, we utilize HXMT data, while both AstroSat and HXMT observations are analyzed for SwiftJ1658.2-4242. Type-C QPOs observed in harder states (LHS, HIMS; $F_{nth}\ge0.4$) exhibit positive lag for low-inclination sources ($i<50^{\circ}$), whereas it generally exhibits negative lag for high-inclination sources ($i>60^{\circ}$), except XTEJ1550-564, SwiftJ1727.8-1613, H1743-322 (2003 outburst) and GROJ1655-40. Notably, type-A QPOs exhibit negative lags ($\sim1-10$ms) regardless of source inclination, while type-B QPOs show positive lags in low-inclination sources, and both positive and negative lags ($\sim1-15$ms) in high-inclination sources, typically occurring in SIMS ($F_{nth}\lesssim0.45$). Systematic appearance of type-A QPOs preceding radio flares in several sources suggests that type-A QPOs indicate telltale signs of jet ejection, while type-B QPOs are closely linked with radio flares (i.e., transient jets). Present findings suggest the corona evolves from a radially extended to a vertically elongated structure during the type-C to type-B transition via type-A QPOs, with type-B QPOs linked to radially compact or vertically extended coronal geometries, resembling jet ejection. The strong radio-X-ray luminosity correlation seems to provide compelling evidence of accretion-powered jets. Finally, we find that jets in SIMS are moderately relativistic in nature with velocities $\gtrsim 0.3-0.8c$ in BH-XRBs under consideration.

Figures

Figures reproduced from arXiv: 2507.03644 by the authors.

Figure 1
Figure 1. Evolution of (a) bolometric (1 − 100 keV) X-ray flux in low inclination sources such as GX 339 − 4 (outbursts in 2002, 2006 and 2010 represented by red, cyan and blue symbols, respectively), 4U 1543 − 47 (orange), Swift J1753.5 − 0127 (yellow), XTE J1752 − 223 (pink) and XTE J1650 − 500 (light green) and (c) in high inclination sources such as XTE J1859 + 226 (red), H1743 − 322 (2009 outburst) (cyan), XTE J1550 − 56… view at source ↗
Figure 3
Figure 3. Evolution of (a) PDS (scaled for better clarity), (b) time lag (open circle) corresponding to different types of QPOs, and (c) bolometric X-ray flux (open circle) and Radio flux in 1.4 − 1.66 GHz (asterisk) near flare F1 (MJD 51467.9) of XTE J1859+226. Different colors denote various types of QPO (green: type-A, blue: type-B, red: type-C and purple: type-C*). See the text for details. transits from HIMS to SIMS, a t… view at source ↗
Figure 2
Figure 2. Evolution of (a) Radio flux in 1.4 − 1.66 GHz (asterisk), (b) bolometric X-ray flux (1−100 keV), (c) Flux ratios (normalized disc flux (triangle) and normalized Comptonized flux (diamond)), (d) photon index (Γ), (e) covering fraction (cov frac), (f) centroid frequency of QPO (νQPO), (g) QPO rms (rmsQPO), (h) total rms (rmsTotal), and (i) time lag at QPO frequency between energy range 6 − 15 keV and 2 − 6 keV of XTE … view at source ↗
Figures from the paper (10 more)
Figure 4
Figure 4. Figure 4: Same as [PITH_FULL_IMAGE:figures/full_fig_p009_4.png]
Figure 5
Figure 5. Figure 5: Evolution of (a) PDS (scaled for better clarity), (b) time lag (open circle) corresponding to different types of QPOs, and (c) bolometric X-ray flux (open circle) and Radio flux at 4.8 GHz (asterisk) near flares (MJD 52408.31) of GX 339−4. Different col￾ors denote vari…
Figure 6
Figure 6. Figure 6: Evolution of QPO rms (rmsQPO%) with time in GX 339 − 4 (i ∼ 50◦), 4U 1543 − 47 (i ∼ 36◦), XTE J1752 − 223 (i ∼ 35◦), XTE J1650 − 500 (i ≥ 47◦), Swift J1753.5 − 0127 (i ≥ 40◦), XTE J1859 + 226 (i ∼ 65◦), H1743 − 322 (i ∼ 75◦), XTE J1550−564 (i ∼ 74◦), Swift J1727.8−1613…
Figure 7
Figure 7. Figure 7: Variation of time lag with Fnth for (upper panel) low inclination sources (GX 339 − 4, 2002 outburst: Diamond, 2007 outburst: octagon, 2010 outburst: Cross, 4U 1743 − 47: Triangle, XTE J1752 − 223: Asterisk, XTE J1650 − 500: Hexagon, Swift J1753.5 − 0127: Inverted Tria…
Figure 8
Figure 8. Figure 8: Evolution of time lag with energy in GX 339−4 (i ∼ 50◦), 2002 and 2007 outburst, 4U 1543−47 (i ∼ 36◦ ), XTE J1752−223 (i ∼ 35◦ ), XTE J1650 − 500 (i ≥ 47◦ ), Swift J1753.5 − 0127 (i ≥ 40◦ ), XTE J1859+226 (i ∼ 65◦), H1743−322 (i ∼ 75◦ ), XTE J1550 − 564 (i ∼ 74◦ ) and …
Figure 9
Figure 9. Figure 9: The figure presents the variation of time lag (in millisec￾onds) with radio flux (in mJy) (in panel (a) and (b)) and bolo￾metric X-ray flux (in panel (c) and (d)) for different black hole X-ray binaries. Panels (a) and (c) correspond to low-inclination sources (XTE J17…
Figure 10
Figure 10. Figure 10: Variation of jet velocity (shaded region) with ε (accounts the fraction of energy transferred to jets from disc) for (a) low￾inclination sources such as, GX 339−4 (green for 2002 outburst and grey for 2010 outburst), 4U 1543 − 47 (skyblue), XTE J1752 − 223 (orange), X…
Figure 11
Figure 11. Figure 11: Variation of intrinsic radio luminosity Lint R (opaque) and LR (semi-transparent) observed radio luminosity with X-ray lu￾minosity for GX 339−4 (2002 and 2010 outbursts denoted with diamond and cross), 4U 1543−47 (triangle), XTE J1752−223 (as￾terisk), XTE J1650−500 (h…
Figure 12
Figure 12. Figure 12: Schematic representation of disc-jet scenarios: (I) Corona is radially extended and large in size, (II) Corona is radially extended but smaller in size, (III) Radial extent of corona is reduced and begins to elongate vertically, and (IV) Radial extent of corona is sma…
Figure 13
Figure 13. Figure 13: Correlation between X-ray luminosity and jet velocity. The dashed line represents the best-fit regression, while the shaded regions indicate the 1σ, 2σ and 3σ confidence intervals. The color bar encodes values of Fnth. Individual sources under consideration are marked…

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